Supernova remnant S 147 and its associated neutron star(s)

Gvaramadze, V. V.

doi:10.1051/0004-6361:20054114

Cited by 43 publications

(65 citation statements)

References 40 publications

(87 reference statements)

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“…6 is taken from Gvaramadze (2006) based on Drew et al (2005). We added the white arrow to mark the NS motion as reported by Gvaramadze (2006). It is consistent with the direction from the geometric center of S 147 to the present position of the pulsar as marked by a white plus sign.…”

Section: Detailed Description Of Snrsmentioning

confidence: 99%

“…We added a white arrow to indicate the NS (pulsar PSR J0538+2817) motion according to (Gvaramadze 2006), from the center of the SNR towards the NS (white plus sign). The white line drawn in the east-west direction shows the bilateral symmetry axis of the SNR (for more details see Gvaramadze 2006). The jets' axis that we mark by the double-headed red arrow on the upper panel is based on the lower panel taken from .…”

Section: Detailed Description Of Snrsmentioning

confidence: 99%

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Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Bear

Soker

2018

ApJ

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We measure the angle between the neutron star (NS) natal kick direction and the inferred direction of jets according to the morphology of 12 core collapse supernova remnants (SNR), and find that the distribution is almost random, but missing small angles. The 12 SNRs are those for which we could both identify morphological features that we can attribute to jets and for which the direction of the NS natal kick is given in the literature. Unlike some claims for spin-kick alignment, here we rule out jet-kick alignment. We discuss the cumulative distribution function of the jet-kick angles under the assumption that dense clumps that are ejected by the explosion accelerate the NS by the gravitational attraction, and suggest that the jet feedback explosion mechanism might in principle account for the distribution of jet-kick angles. arXiv:1710.00819v2 [astro-ph.HE]

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Section: Detailed Description Of Snrsmentioning

confidence: 99%

Section: Detailed Description Of Snrsmentioning

confidence: 99%

Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Bear

Soker

2018

ApJ

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“…3). These "well defined nebulae are formed during a brief post-main-sequence phase when a massive star becomes a Wolf-Rayet star or a Luminous Blue Variable star" (Gvaramadze et al 2010). Some of them show a bipolar structure when observed by Spitzer.…”

Section: What Do We Expect To See?mentioning

confidence: 99%

Bipolar H II regions – Morphology and star formation in their vicinity

Deharveng

Zavagno

Samal

et al. 2015

A&A

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Aims. Our goal is to identify bipolar H ii regions and to understand their morphology, their evolution, and the role they play in the formation of new generations of stars.Methods. We use the Spitzer-GLIMPSE, -MIPSGAL, and Herschel-Hi-GAL surveys to identify bipolar H ii regions, looking for (ionized) lobes extending perpendicular to dense filamentary structures. We search for their exciting star(s) and estimate their distances using near-IR data from the 2MASS or UKIDSS surveys. Dense molecular clumps are detected using Herschel-SPIRE data, and we estimate their temperature, column density, mass, and density. MALT90 observations allow us to ascertain their association with the central H ii region (association based on similar velocities). We identify Class 0/I young stellar objects (YSOs) using their Spitzer and Herschel-PACS emissions. These methods will be applied to the entire sample of candidate bipolar H ii regions to be presented in a forthcoming paper.Results. This paper focuses on two bipolar H ii regions, one that is especially interesting in terms of its morphology, G319.88+00.79, and one in terms of its star formation, G010.32−00.15. Their exciting clusters are identified and their photometric distances estimated to be 2.6 kpc and 1.75 kpc, respectively; thus G010.32−00.15 (known as W31 north) lies much closer than previously assumed. We suggest that these regions formed in dense and flat structures that contain filaments. They have a central ionized region and ionized lobes extending perpendicular to the parental cloud. The remains of the parental cloud appear as dense (more than 10 4 cm −3 ) and cold (14-17 K) condensations. The dust in the photodissociation regions (in regions adjacent to the ionized gas) is warm (19-25 K). Dense massive clumps are present around the central ionized region. G010.32-00.14 is especially remarkable because five clumps of several hundred solar masses surround the central H ii region; their peak column density is a few 10 23 cm −2 , and the mean density in their central regions reaches several 10 5 cm −3 . Four of them contain at least one massive YSO (including an ultracompact H ii region and a high-luminosity Class I YSO); these clumps also contain extended green objects (EGOs) and Class II methanol masers. This morphology suggests that the formation of a second generation of massive stars has been triggered by the central bipolar H ii region.It occurs in the compressed material of the parental cloud.

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“…Since both pulsars are not recycled, one should assume either that the binary separation was sufficiently large (so that the wind of the secondary star did not affect the evolution of the first-born pulsar) or that the binary evolved through a double common-envelope phase (see above). VCC04 suggest that the pulsars were born in a wide binary, but in their analysis they draw an erroneous conclusion that the pulsar velocities can be explained by a kick of only 200 km s −1 (see Gvaramadze 2006). One can show, however, that in both the above-mentioned cases the kick imparted by the second SN explosion should be ≥500 km s −1 .…”

Section: Pulsars B2020+28 and B2021+51: Origin In A Common Binarymentioning

confidence: 98%

Separated before birth: pulsars B2020+28 and B2021+51 as the remnants of runaway stars

Gvaramadze

2007

A&A

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Astrometric data on the pulsars B2020+28 and B2021+51 suggest that they originated within several parsecs of each other in the direction of the Cyg OB2 association. It was proposed that the pulsars share their origin in a common massive binary and were separated at the birth of the second pulsar following the asymmetric supernova explosion. We consider a different scenario for the origin of the pulsar pair based on a possibility that the pulsars were separated before their birth and that they are the remnants of runaway stars ejected (with velocities similar to those of the pulsars) from the core of Cyg OB2 due to strong three-or four-body dynamical encounters. Our scenario does not require any asymmetry in supernova explosions. IntroductionMost stars form in dense embedded clusters and reside in binary systems (either primordial or tidal). If both binary components are massive enough, they end their lives as core-collapsed supernovae (SNe). Stellar remnants of SN explosions, usually the neutron stars (NSs), have peculiar velocities at least an order of magnitude higher than the typical velocities of their progenitors, the OB stars (e.g. Gunn & Ostriker 1970). It is believed that the high velocities of NSs are due either to the asymmetry of SN explosions (e.g. Dewey & Cordes 1987) or to the disruption of tight massive binaries following the second (symmetric) SN explosion (e.g. Iben & Tutukov 1996). The progress in measuring the proper motions and parallaxes of NSs (pulsars) allows their peculiar (transverse) velocities to be determined with high precision and makes it possible to trace their trajectories back to the parent star clusters (e.g. Hoogerwerf et al. 2001;Chatterjee et al. 2005). Recently Vlemmings et al. (2004; hereafter VCC04) have used the high-precision astrometric data (proper motions and parallaxes) for two dozen pulsars to determine their trajectories in the Galactic potential and to search for pairs with a common origin. They discovered that two pulsars from their sample (presently separated by ∼23• ) originated within several parsecs of each other in the direction of the Cyg OB2 association. VCC04 interpret their discovery as an indication that the progenitors of both pulsars, B2020+28 and B2021+51, were the members of a common massive binary and suggest that the pulsars were separated at the birth of the second one following the asymmetric SN explosion.In this Letter we explore a different scenario for the origin of B2020+28 and B2021+51. We suggest that these pulsars were separated before their birth and that they are the remnants of runaway stars ejected (with velocities similar to those of the pulsars) from the parent star cluster due to the strong three-or fourbody dynamical encounters. Our scenario does not require any asymmetry in SN explosions. Pulsars B2020+28 and B2021+51: origin in a common binaryThe main result presented in VCC04 is that B2020+28 and B2021+51 originated within several parsecs of each other. VCC04 derived the most likely three-dimensional peculiar veloci...

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Supernova remnant S 147 and its associated neutron star(s)

Cited by 43 publications

References 40 publications

Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Bipolar H II regions – Morphology and star formation in their vicinity

Separated before birth: pulsars B2020+28 and B2021+51 as the remnants of runaway stars

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